Download EEn.1.1 Explain the Earth`s role as a body in space. EEn

EEn.1.1 Explain the Earth’s role as a body in space. EEn.1.1.1 Explain the Earth’s motion through space, including precession, nutation, the barycenter, and its path about the galaxy. EEn.1.1.1 • Explain the origin of the Earth’s motion based on the origin of the galaxy and its solar system. • Explain Precession­change in direction of the axis, but without any change in tilt ­this changes the stars near (or not near) the Pole, but does not affect the seasons (as long as the angle of 23.5 degrees stays the same) • Explain nutation­wobbling around the precessional axis (This is a change in the angle­½ degree one way or the other. This occurs over an 18 year period and is due to the Moon exclusively. This would very slightly increase or decrease the amount of seasonal effects.) • Explain relative motion of the Earth in the solar system, the solar system in the galaxy, and the galaxy in the universe­
including the expanding nature of the universe; Orbital motion (Earth around the Sun­ once/year, seasons depend upon an approximate 23.5 degree tilt); Rotation around our axis (day/night,) • Explain planetary orbits, especially that of the Earth, using Kepler’s laws. • Explain barycenter­the point between two objects where they balance each other
(For example, it is the center of mass where two or more celestial bodies orbit each other. When a moon orbits a planet, or a planet orbits a star, both bodies are actually orbiting around a point that lies outside the center of the primary (the larger body). For example, the moon does not orbit the exact center of the Earth, but a point on a line between the Earth and the Moon approximately 1,710 km below the surface of the Earth, where their respective masses balance. This is the point about which the Earth and Moon orbit as they travel around the Sun. • 1
EEn.1.1.2 Explain how the Earth’s rotation and revolution about the Sun affect its shape and is related to seasons and tides. • Describe daily changes due to rotation, seasonal changes due to the tilt and revolution of the Earth, and tidal impact due to the gravitational interaction between the Earth and moon. • Develop a cause and effect model for the shape of the Earth explaining why the circumference around the equator is larger than that around the poles. EEn.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. EEn.1.1.3 • Compare combustion and nuclear reactions (fusion and fission) on a conceptual level. Identify fusion as the process that produces radiant energy of stars. • Identify the forms of energy (electromagnetic waves) produced by the sun and how some are filtered by the atmosphere (X­rays, cosmic rays, etc.). • Summarize how energy flows from the sun to the Earth through space. EEn.1.1.4 Explain how incoming solar energy makes life possible on Earth. EEn.1.1.4 • Explain how the tilt of the Earth’s axis results in seasons due to the amount of solar energy impacting the Earth’s surface. • Explain differential heating of the earth’s surface (water temperature vs. land temperature) • Explain how solar energy is transformed into chemical energy through photosynthesis. • Explain how the earth’s magnetic field protects the planet from the harmful effects of radiation.
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• Explain the origin of the Earth’s motion based on the origin of the galaxy and its solar system
christophercrockett.com
Movement Of the Earth's Axis
1. Nutation 2. Precession
3. Rotation
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• Explain nutation­wobbling around the precessional axis (This is a change in the angle­½ degree one way or the other. This occurs over an 18 year period and is due to the Moon exclusively. This would very slightly increase or decrease the amount of seasonal effects.) Nutation
James Bradley announced his discovery of nutation in 1748.
Nutation is, in astronomy, a small irregularity in the precession of the equinoxes.
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• Explain nutation­wobbling around the precessional axis Nutation
~ is a rocking, swaying, or nodding motion in the Earth’s axis of rotation
~ In the case of Earth , the principal sources of tidal force are the Sun and Moon which continuously change location relative to each other and thus cause nutation in Earth's axis
~ The largest component of Earth's nutation has a period of 18.6 years,
­wobbling around the precessional axis (This is a change in the angle­½ degree one way or the other. This occurs over an 18 year period and is due to the Moon exclusively. This would very slightly increase or decrease the amount of seasonal effects.) 5
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is caused by the gravitational pull of the Sun and the Moon on the Earth.
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• Explain Precession­change in direction of the axis, but without any change in tilt ­this changes the stars near (or not near) the Pole, but does not affect the seasons (as long as the angle of 23.5 degrees stays the same) 6
• Explain Precession­change in direction of the axis, but without any change in tilt ­this changes the stars near (or not near) the Pole, but does not affect the seasons (as long as the angle of 23.5 degrees stays the same) 7
• Explain Precession­change in direction of the axis, but without any change in tilt ­this changes the stars near (or not near) the Pole, but does not affect the seasons (as long as the angle of 23.5 degrees stays the same) 8
• Describe daily changes due to rotation,
Rotation of the Earth's Axis
Earth Spinning in Space on its Axis
Spins counterclockwise
Speed 1675 km/h or 465 meters/second. That’s 1,040 miles/hour. Want to do the calculation for yourself? The at the equator is 40,075 km. And the length of time the Earth takes to complete one full turn on its axis is 23.93 hours. Then we divide the length of a day into the distance a point on the equator travels in that period: 40,075 km/23.93 hours = 1,675 km/hour, 465 meters/second.
Causes night and day
: http://www.universetoday.com/26623/how­fast­does­the­earth­rotate/#ixzz2tJQy04bk <http://www.universetoday.com/26623/how­fast­does­the­earth­rotate/>
http://www.polaris.iastate.edu/NorthStar/Unit3/unit3_sub1.htm
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Describe daily changes due to rotation,
Solar Days and Sidereal Days
Solar time is measured with respect to the Sun's apparent motion in the sky. The clocks we use are based on this motion. The apparent motion of the Sun across the sky is actually caused by the rotation of the Earth. Our clocks measure the length of time required for the Earth to rotate once with respect to the Sun. From our perspective, the Sun revolves around the Earth every 24 hours. This period is known as a solar day. Sidereal time is measured with respect to the apparent motion of the 'fixed' stars in the sky due to the Earth's rotation.
While the Earth is rotating on its axis it is also moving along its orbit around the Sun.
Over the course of a day the Earth moves about one degree along its orbit (360 degrees in a full orbit divided by 365.25 days in a year is about one degree). Therefore, from our perspective, the Sun moves about one degree from west to east with respect to the 'fixed' stars. All of this means that according to our clocks, which are based on solar time, a given star will rise or set about four minutes earlier each day
(the Earth rotates 15 degrees in one hour, i.e. 360/24, so one degree of rotation is equivalent to about four minutes of time). For example, a star that rises at 9:00pm (21:00) tonight will rise at 8:56 pm (20:56) tomorrow and at 8:52pm (20:52) the next night. One month later that star will rise or set two hours earlier. In other words, from our perspective, the stars revolve around the Earth in only 23 hours and 56 minutes. This period is known as a sidereal day. http://community.dur.ac.uk/john.lucey/users/e2_solsid.html
Sidereal Time
Astronomers make use of the sidereal day, which is the time required for the Earth to make one complete rotation (360°) with respect to the stars.
The "day" that is used in everyday life is the solar day, which is (approximately)
the time from when the Sun is highest in the sky to when it is again highest in the sky. Because the Earth moves around the Sun as it rotates, in one solar day the Earth must rotate through about 361°. A solar day is about 4 minutes longer than a sidereal day. http://csep10.phys.utk.edu/astr161/lect/time/timekeeping.html
http://bcs.whfreeman.com/universe7e/content/ch02/0203003.html
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Describe daily changes due to rotation,
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Describe the tidal impact due to the gravitational interaction between the Earth and moon. Moon's Rotation Around the Earth
http://www.youtube.com/watch?v=OZIB_leg75Q
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Describe the tidal impact due to the gravitational interaction between the Earth and moon. Tides
Changes in the elevation of the ocean surface
Force that moves the ocean
­Sun and Moon's gravity causes tides on Earth
* Gravitational force between Earth and Moon and Sun
Every 6 hours time oceans rise and fall.
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Describe the tidal impact due to the gravitational interaction between the Earth and moon. Effect the Moon's Rotation has on Earth's Tides
The tides at a given place in the Earth's oceans
occur about an hour later each day. Since the Moon passes overhead about an hour later each day, it was long suspected that the Moon
was associated with tides. Newton's Law of Gravitation provided a quantitative understanding of that association
http://www.onr.navy.mil/focus/ocean/motion/tides2.htm
Read Article and Take Quiz
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Describe the tidal impact due to the gravitational interaction between the Earth and moon. Tides The moon is a major influence on the Earth’s tides,
but the sun also generates considerable tidal forces. Solar tides are about half as large as lunar tides and are expressed as a variation of lunar tidal patterns, not as a separate set of tides.
http://oceanservice.noaa.gov/education/kits/tides/tides06_variations.html
When the sun, moon, and Earth are in alignment (at the time of the new or full moon), the solar tide has an additive effect on the lunar tide, creating extra­high high tides, and very low, low tides­both commonly called spring tides. **** Spring tides are not named from the season but from "spring forward") This occurs twice each month, when the moon is full and new.
At the first quarter moon ~ 1 week after new moon and
third quarter moon ~ 1 week after the full moon, the sun and moon are at a 45° angle to each other and the solar tide partially cancels out the lunar tide and produces moderate tides known as neap tides.
During each lunar month, two sets of spring tides and two sets of neap tides occur (Sumich, J.L., 1996).
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Describe the tidal impact due to the gravitational interaction between the Earth and moon. csep10.phys.utk.edu
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http://en.wikipedia.org/wiki/Tide
Describe the tidal impact due to the gravitational interaction between the Earth and moon. 18
In this diagram, you can see that the moon's gravitational force pulls on water in the oceans so that there are "bulges" in the ocean on both sides of the planet.
The moon pulls water toward it, and this causes the bulge toward the moon.
The bulge on the side of the Earth opposite the moon is caused by the moon "pulling the Earth away" from the water on that side.
If you are on the coast and the moon is directly overhead, you should experience a high tide.
If the moon is directly overhead on the opposite side of the planet, you should also experience a high tide.
During the day, the Earth rotates 180 degrees in 12 hours. The moon, meanwhile, rotates 6 degrees around the earth in 12 hours. The twin bulges and the moon's rotation mean that any given coastal city experiences a high tide every 12 hours and 25 minutes or so.
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Explain barycenter­the point between two objects where they balance each other
(For example, it is the center of mass where two or more celestial bodies orbit each other.
When a moon orbits a planet, or a planet orbits a star, both bodies are actually orbiting around a point that lies outside the center of the primary (the larger body). For example, the moon does not orbit the exact center of the Earth, but a point on a line between the Earth and the Moon approximately 1,710 km below the surface of the Earth, where their respective masses balance. This is the point about which the Earth and Moon orbit as they travel around the Sun. Barycenter
The exact center of all the material (that is, mass) that makes up an object‐whether a planet or a pencil‐is called its "center of gravity."
it is the center of mass where two or more celestial bodies orbit each other. When a moon orbits a planet, or a planet orbits a star , both bodies are actually orbiting around a point that is not at the center of the primary (the larger body). For example, the Moon does not orbit the exact center of the Earth , but a point on a line
between the center of the Earth and the Moon, approximately 1,710 km below the surface of the Earth, where their respective masses balance. This is the point about which the Earth and Moon orbit as they travel around the sun
http://www.youtube.com/watch?v=uGBANgbRkws
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Explain barycenter­the point between two objects where they balance each other
The Earth ­­ Moon Barycenter
the point between two objects where they balance each other as they orbit each other
http://scienceprojectideasforkids.com/2010/barycenter­of­the­earth­moon­system/
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Explain barycenter­the point between two objects where they balance each other
Sun ­ Earth ­ Moon Barycenter
http://www.youtube.com/watch?v=W47Wa7onrIQ
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Summarize that the Sun is not stationary in our solar system. It actually moves as the planets tug on it, causing it to orbit the solar system's barycenter.
The Sun never strays too far from the solar system barycenter. These time periods relate to the motion of the Sun around the centre of mass of the solar system. Here’s a plot of the motion so you can get an idea of what this is about.
This is caused by the changing positions of the planets as they orbit, pulling the Sun around the centre of mass or solar system barycentre.
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Image Courtesey of Carsten Anholm and Geoff Sharp
Summarize that the Sun is not stationary in our solar system. It actually moves as the planets tug on it, causing it to orbit the solar system's barycenter.
The Sun never strays too far from the solar system barycenter. 24
Describe seasonal changes due to the tilt and revolution of the Earth, Revolution
Orbital motion (Earth around the Sun­ once/year, seasons depend upon an approximate 23.5 degree tilt); Earth Revolving Around the Sun
Speed: 67, 062 miles per hour
Time: 365.25 days ~ 1 year
Reason for the Seasons
Earth has seasons because its axis doesn't stand up straight. (23.5 degree tilt)
http://astro.unl.edu/naap/motion1/animations/seasons_ecliptic.html
http://csep10.phys.utk.edu/astr161/lect/time/timekeeping.html
http://www.youtube.com/watch?v=48cKCKnJ7jA
How fast does earth move around the sun? 25
Describe seasonal changes due to the tilt and revolution of the Earth, Re
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12 hours of daylight and darkness on entire planet
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Describe seasonal changes due to the tilt and revolution of the Earth, http://aspire.cosmic­ray.org/Labs/Tides/critical_speed.html
Do simulator Answer Queswtions on Separate Paper
http://d1jqu7g1y74ds1.cloudfront.net/wp­content/uploads/2009/12/tilts_big.jpg
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Describe seasonal changes due to the tilt and revolution of the Earth, Revolution
http://astro.unl.edu/naap/motion1/animations/seasons_ecliptic.html
http://aa.usno.navy.mil/data/docs/EarthSeasons.php
Equinoxes ~ Equal time
12 hours of daylight and darkness on entire planet
~ mark the beginning of spring and fall. March 21st September 21st
June 21st December 21st
mark the beginning of summer and winter. Solstices ~ Longest day and longest night 28
Describe seasonal changes due to the tilt and revolution of the Earth,
From Wikipedia, the free encyclopedia
An equinox occurs twice a year (around 20 March and 22 September), when the plane of Earth's equator passes the center of the Sun. At this time the tilt of the Earth 's axis is inclined neither away from nor towards the Sun .
The term equinox can also be used in a broader sense, meaning the date when such a passage happens. The name "equinox" is derived from the Latin aequus (equal) and nox (night), because around the equinox, night and day are about equal length.
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Describe seasonal changes due to the tilt and revolution of the Earth,
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Kepler's Laws <KeplersLaws.jpg> Using the extensive collection of planetary positions measured by Tycho Brahe over several decades,
~Kepler was able to distill these thousands of observations to 3 Laws of Planetary Motion.
~The first Law says that the orbits of planets around the Sun are ellipitcal in shape, NOT circular (or circle with epicycles and other such nonsense.)
~The second Law is shown graphically in the next viewgraph. This Law is just a statements of the conservation of angular momentum, but Kepler did not know about this concept.
~The third Law is a quantitative relationship between the orbital period (time for a body to orbit Sun once) and the size of the orbit of the body (expressed as the semimajor axis ­ a ­ of the orbit).
~ Note that these Laws were expressed by Kepler around 400 years ago!!
~ Kepler did not understand the physics behind his laws, but (somehow!)
~ was able to see the simple basic patterns that could account for the observations of planetary positions. ~ Of course, the planetary positions are measured from the Earth, which is also moving!
~ Certainly this is one of the most stunning intellectual acheivements of mankind. 31
• Explain planetary orbits, especially that of the Earth, using Kepler’s laws.
Explain relative motion of the Earth in the solar system, the solar system in the galaxy, and the galaxy in the universe­
including the expanding nature of the universe; Orbital motion Kepler's Laws.
Kepler's Laws
Johannes Kepler, working with data painstakingly collected by Tycho Brahe without the aid of a telescope, developed three laws which described the motion of the planets across the sky. 1. The Law of Orbits: All planets move in elliptical orbits, with the sun at one focus.
2. The Law of Areas: A line that connects a planet to the sun sweeps out equal areas in equal times. 3. The Law of Periods: The square of the period of any planet is proportional to the cube of the semimajor axis of its orbit. Kepler's laws were derived for orbits around the sun, but they apply to satellite orbits as well. 32
First Law: The Law of Orbits: 33
2. The Law of Areas:
3. The Law of Periods: 34
First Law: The Law of Orbits: Keplers first law of planetary motion is that each planet orbits the Sun in an ellipse.
The Sun is at one of the foci of the ellipse, NOT at the center of the ellipse
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First Law: The Law of Orbits: 36
First Law: The Law of Orbits: Kepler's First Law
Planets move in elliptical orbits with the Sun not at the center of the ellipse, but at one focus (the other focus is empty). It’s a deceptively simple law that took astonishing insight and five years of hard work.
http://oneminuteastronomer.com/8626/keplers­laws/
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First Law: The Law of Orbits: Draw an ellipse with string
http://www.mathopenref.com/constellipse1.html
http://www.google.com/imgres?q=earth's%20eccentricity&safe=active&sa=X&biw=1024
&bih=557&tbm=isch&tbnid=YxEAlfeZiLgdpM%3A&imgrefurl=http%3A%2F%
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VM&imgurl=http%3A%2F%2Fwww.soes.soton.ac.uk%2Fstaff%2Fejr%2FDarkMed%2F6­
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1547&page=3&start=20&ndsp=12&ved=0CK4BEK0DMBw
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Kepler's second law of planetary motion describes the speed of a planet traveling in an elliptical orbit around the sun. It states that a line between the sun and the planet sweeps equal areas in equal times. Thus, the speed of the planet increases as it nears the sun and decreases as it recedes from the sun.
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2. The Law of Areas:
Kepler’s Second Law
~ A planet's distance from the Sun changes during an orbit.
~Kepler noticed that planets seemed to speed up in their orbits when they are closer to the Sun and slow down when they’re further away.
Kepler had to quantify this motion, and did so by stating that ”
~a line joining a planet and the Sun sweeps out equal areas during equal intervals of time.” <http://oneminuteastronomer.com/wp­content/uploads/2013/06/kepler2.gif> <http://oneminuteastronomer.com/wp­content/uploads/2013/06/kepler2.gif>
Kepler’s 2nd Law: The line from the Sun to a planet sweeps out equal areas in equal times.
“Who cares”, you might ask? Well… this doesn’t affect your everyday life
and enjoyment of the night sky, but Kepler’s 2nd Law is
a) Critical for predicting where we can see planets in the sky, b) A direct consequence of the great universal law of “conservation of energy”
. As a planet gets closer to the Sun, it has less “potential energy” and more “kinetic energy”, and as it moves away from the Sun, it has the opposite. Without this law, we’d still be scratching our head about where and when the planets appear in the night sky.
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2. The Law of Areas:
Kepler's second law of planetary motion describes the speed of a planet traveling in an elliptical orbit around the sun. It states that a line between the sun and the planet sweeps equal areas in equal times. Thus, the speed of the planet increases as it nears the sun and decreases as it recedes from the sun.
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2. The Law of Areas:
Kepler's second law relates the speed of a planet's orbit to its distance from the Sun.
A planet has the most gravitational potential energy and the least kinetic energy when it is farthest from the Sun.
It has the least gravitational potential energy and the most kinetic energy when it is closest to the Sun. The orbit is a continuous conversion of the two types of energy.
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2. The Law of Areas:
Keplers second law (the "equal area" law) states that the area swept out by the line between planet and Sun
is equal for equal time. The planet would take the same amount of TIME to go from A to B as from B to C, etc. For example, the area of the cross­hatched region between points A, B and Sun would be equal to the
cross­hatched area between point H, I and the Sun. As the distance between A and B along the orbit is larger than the distance between H and I along the orbit, but the time the same, the planet
must move faster between A and B than between H and I. hildaandtrojanasteroids.net
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2. The Law of Areas:
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2. The Law of Areas:
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Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
Kepler's Third Law
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3. The Law of Periods:
Kepler's third law ­ sometimes referred to as the law of harmonies ­ compares the orbital period and radius of orbit of a planet to those of other planets.
Unlike Kepler's first and second laws that describe the motion characteristics of a single planet,
the third law makes a comparison between the motion characteristics of different planets.
The comparison being made is that the ratio of the squares of the periods to the cubes of their average distances
from the sun is the same for every one of the planets.
As an illustration, consider the orbital period and average distance from sun (orbital radius)
for Earth and mars as given in the table below.
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3. The Law of Periods:
a= average distance of the planet to the sun
p = time period of the orbit
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spaceodyssey.dmns.org/media/3304/keplerslawsofplan
Kepler's 3rd law is a mathematical formula. It means that if you know the period of a planet's orbit (P = how long it takes the planet to go around the Sun), then you can determine that planet's distance from the Sun
(a = the semimajor axis of the planet's orbit). It also tells us that planets that are far away from the Sun have longer periods than those close to the Sun. They move more slowly around the Sun. compares the orbital period and radius of orbit of a planet to those of other planets. Unlike Kepler's first and second laws that describe the motion characteristics of a single planet, the third law makes a comparison between the motion characteristics of different planets.
The comparison being made is that the ratio of the squares of the periods
to the cubes of their average distances from the sun is the same for every one of the planets. As an illustration, consider the orbital period and average distance from sun
(orbital radius) for Earth and mars as given in the table below.
http://www.youtube.com/watch?v=dRT3m2Wzyh4
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s: Observe that the T2/R3 ratio is the same for Earth as it is for mars. In fact, if the same T2/R3 ratio is computed for the other planets, i
t can be found that this ratio is nearly the same value for all the planets (see table below).
Amazingly, every planet has the same T2/R3 ratio.
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0.39
0.98
Venus
.615
0.72
1.01
Earth
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1.00
1.00
Mars
1.88
1.52
1.01
Jupiter
11.8
5.20
0.99
Saturn
29.5
9.54
1.00
Uranus
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19.18
1.00
Neptune
165
30.06
1.00
Pluto
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39.44
1.00
http://www.physicsclassroom.com/class/circles/u6l4a.cfm
(NOTE: The average distance value is given in astronomical units where 1 a.u. is equal to the distance from the earth to the sun ­ 1.4957 x 1011 m. The orbital period is given in units of earth­years where 1 earth year is the time required for the earth to orbit the sun ­ 3.156 x 107 seconds. )
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EEn.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. 53
En.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. EEn.1.1.3 • Compare combustion and nuclear reactions (fusion and fission) on a conceptual level.
Identify fusion as the process that produces radiant energy of stars. • Identify the forms of energy (electromagnetic waves) produced by the sun and how some are 54
En.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. http://www.northlandprep.org/wp­content/uploads/2012/03/the_sun_worksheet.pdf
http://www.youtube.com/watch?v=32KVGQy3bMY
How the Sun Works
http://science.howstuffworks.com/sun2.htm
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EEn.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. How does the Sun produce energy? The Sun produces energy by the nuclear fusion of hydrogen into helium in its core.
What that means is that, since there is a huge amount of hydrogen in the core, these atoms stick together and fuse into a helium atom. This energy is then radiated out from the core and moves across the solar system.
Read more: http://www.universetoday.com/75803/how­does­the­sun­produce­energy/#ixzz2tlJKpBjb <http://www.universetoday.com/75803/how­does­the­sun­produce­energy/>
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• Identify the forms of energy (electromagnetic waves) produced by the sun and how some are filtered by the atmosphere (X­rays, cosmic rays, etc.). What is Radiation?
http://radbelts.gsfc.nasa.gov/outreach/space_radiation.html
http://hps.org/publicinformation/ate/faqs/whatisradiation.html
http://www.qrg.northwestern.edu/projects/vss/docs/space­environment/2­what­is­
electromagnetic­radiation.html
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• Identify the forms of energy (electromagnetic waves) produced by the sun and how some are filtered by the atmosphere (X­rays, cosmic rays, etc.). What is Radiation?
The word 'radiation' has to do with energy moving through space. Energy traveling in the form of vibrations ~ waves
There are many forms of radiation that astronomers and physicists know about
E
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Electromagnetic Waves
Transverse Waves
­ The movement of the matter's particles are perpendicular to the motion of the wave (up and down)
­ The medium moves at right angles to the direction the wave travels
­ water waves, electromagnetic waves
*** Electromagnetic waves do not need a medium to travel
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Electromagnetic Waves
movement =
Transverse Waves
­ The movement of the matter's particles are perpendicular to the motion of the wave
The diagram illustrates the motion of a transverse wave. Light waves are examples of transverse waves: they undulate at right angles to the direction of travel and are characterized by alternating crests and troughs. Simple water waves, such as the ripples produced when a stone is dropped into a pond,
are also examples of transverse waves.(Image © RM) Image 2 of 2
http://www.talktalk.co.uk/reference/encyclopaedia/hutchinson/m0006049.html
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Wave Movement
Transverse
The movement of the matter's particles are
perpendicular to the motion of the wave
water, electromagnetic
Longitudinal Waves
particles vibrate in the same direction
as or parallel to the wave
Sound and seismic waves
The diagram illustrates the motion of a longitudinal wave. Sound, for example, travels through air in longitudinal waves:
the waves vibrate back and forth in the direction of travel. In the compressions the particles are pushed together, and in the rarefactions they are pulled apart.(Image © RM) Image 1 of 2
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D. Electromagnetic Waves
1. Description ­ Transverse Waves
­ Produced by electrically charged particles
­ called photons ­ waves radiate from photons
­ do not need a medium to travel through
­ can travel through a vaccum
­ have fluctuating magnetic and electric fields
­ perpendicular to each other and perpendicular to the direction the light travels
/www.geo.mtu.edu/rs/back/spectrum/
62
EEn.1.1.3 • Identify the forms of energy (electromagnetic waves) produced by the sun and
how some are filtered by the atmosphere (X­rays, cosmic rays, etc.). http://www.google.com/imgres?sa=X&biw=1024&bih=557&tbm=isch&tbnid=18Fs­8JjgP_4pM%3A&imgrefurl=http%3A%2F%2Fwww.docstoc.com%2Fdocs%2F79727858%2FElectromagnetic­Spectrum­Worksheet&docid=
45AQs1WR23t8yM&imgurl=http%3A%2F%2Fimg.docstoccdn.com%2Fthumb%2Forig%2F79727858.png&w=1275&h=1650&ei=pSkNU4mSKvPW0gH_o4G4Bg&zoom=1&iact=rc&dur=1000&page=1&start=0&ndsp=8&ved=
0CFIQrQMwAA
http://www.sciencewithmrjones.com/downloads/astronomy/universe/electromagnetic_spectrum_&_light_­_webquest.pdf
http://www.google.com/#q=school.discoveryeducation.com%2Flessonplans%2Finteract%2Felectromagneticspectrum.html
electromagnetic spectrum
imagine.gsfc.nasa.gov
63
EEn.1.1.3 • Identify the forms of energy (electromagnetic waves) produced by the sun and how some are filtered by the atmosphere (X­rays, cosmic rays, etc.). http://delloyd.50megs.com/moreinfo/spectrum.html Use website to list facts in EM
The Electromagnetic Spectrum of Radiation
All of these waves are electric and magnetic forces
All have speed 186,000 miles per second = c = speed of light !
300,000 km/sec
They move through vacuum, and do not need a ' carrier'.
Speed decreases after entering materials.
The only difference between them is their wavelength,
which is directly related to the amount of energy the waves carry.
The shorter the wavelength of the radiation, the higher the energy. 64
• Identify the forms of energy (electromagnetic waves) produced by the sun and
how some are filtered by the atmosphere (X­rays, cosmic rays, etc.). • Summarize how energy flows from the sun to the Earth through space. http://imagine.gsfc.nasa.gov/docs/science/know_l1/emspectrum.html
EEn.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. http://imagine.gsfc.nasa.gov/docs/science/quiz_l1/emspectrum_quiz.html
65
Compare combustion and nuclear reactions (fusion and fission) on a conceptual level.
Identify fusion as the process that produces radiant energy of stars. • Compare combustion and nuclear reactions (fusion and fission) on a conceptual level. Identify fusion as the process that produces radiant energy of stars. http://www.youtube.com/watch?v=pusKlK1L5To
Fusion
http://www.meridianschools.org/MHS/TeachersStaff/MP/Nawrocki
/AssignmentsInformation/Nuclear%20Fission%20vs%20Fusion.pdf
http://www.youtube.com/watch?v=mBdVK4cqiFs
Fission
http://www.rsec.psu.edu/pages/education/lessons/Combustion%20Fission%20Fusion.pdf
lesson
66
• Compare combustion and nuclear reactions (fusion and fission) on a conceptual level.
Identify fusion as the process that produces radiant energy of stars. Combustion
http://web.mnstate.edu/marasing/CHEM102/Chapter%20Notes/Ch_04%20ho.pdf
http://fusioned.gat.com/education_notebook/images/pdf/fusion_workbook.pdf
workbook on fusion and fission
67
EEn.1.1.4 Explain how incoming solar energy makes life possible on Earth. EEn.1.1.4 • Explain how the tilt of the Earth’s axis results in seasons due to the amount of solar energy impacting the Earth’s surface. • Explain differential heating of the earth’s surface (water temperature vs. land temperature) • Explain how solar energy is transformed into chemical energy through photosynthesis. • Explain how the earth’s magnetic field protects the planet from the harmful effects of radiation.
68
• Summarize how energy flows from the sun to the Earth through space. EEn.1.1.3 Explain how the sun produces energy which is transferred to the Earth by radiation. http://science­edu.larc.nasa.gov/EDDOCS/radiation_facts.html
69
EEn.1.1.4 Explain how incoming solar energy makes life possible on Earth. • Explain how the tilt of the Earth’s axis results in seasons due to the amount of solar energy impacting the Earth’s surface. 70
Describe seasonal changes due to the tilt and revolution of the Earth, Re
Axi
s is
Win
n
o
i
ut
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o
v
Autumnal Equinox
Re
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Wi
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tilte
So
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ter i
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Sum
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orth
Sol
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way
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ern
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un
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Hemis r in Northe
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em
isph
stice
North
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towar rn axis is t
d the
sun ilted Su
ere
Vernal Equinox
Axis is not tilted toward the sun
12 hours of daylight and darkness on entire planet
nationsonline.org
71
EEn.1.1.4 Explain how incoming solar energy makes life possible on Earth. • Explain differential heating of the earth’s surface (water temperature vs. land temperature) http://www.ucar.edu/learn/1_1_2_5t.htm
http://www.ucmp.berkeley.edu/education/dynamic/session4/sess4_act3.htm
72
• Explain how solar energy is transformed into chemical energy through photosynthesis • Explain how the earth’s magnetic field protects the planet from the harmful effects of radiation.
1.1.4• Explain how solar energy is transformed into chemical energy through photosynthesis
Concept 1: An Overview of Photosynthesis Photosynthesis converts light energy into the chemical energy of sugars and other organic compounds. This process consists of a series of chemical reactions
that require carbon dioxide (CO2) and water (H2O)
and store chemical energy in the form of sugar.
Light energy from light drives the reactions. Oxygen (O2) is a byproduct of photosynthesis
and is released into the atmosphere. The following equation summarizes photosynthesis
sunlight + 6 CO2 + 6 H2O → 6(CH2O) + 6 O2 sugar
http://www.phschool.com/science/biology_place/biocoach/photosynth/electro.html
shows diagram of photosynthesis
73
• Explain how the earth’s magnetic field protects the planet from the harmful effects of radiation
http://www.windows2universe.org/earth/Magnetosphere/overview.html
Explain how the earth’s magnetic field protects the planet from the harmful effects of radiation
74
Attachments
Kepler's Laws.pdf